0320042

Black Holes (BH) in the thick disc and/or halo of the Milky Way galaxy appear sporadically as X-ray Novae (XN) with very hard spectra. The origin of these objects are among the most intriguing problems in high-energy astrophysics: they could have been shot out from the Galactic Plane (GP) or be pristine BH formed in the galactic halo before the galactic disc was formed. At latitudes |b| > 5 deg BH XN are likely to be close to the Sun bright optically unobscured the compact radio counterpart is subject to low interstellar scattering. The proposed study will allow to: 1) probe the connection between accretion disc instabilities and the formation of relativistic jets in all wavelength bands 2) know whether the radio infrared and optical non-thermal components and the gamma-ray events originate -as recently found in quasars- within the same shocked area downstream the relativistic jet and 3) determine the space velocity of the binary centre of mass to know where these BH come from. The discovery of XTE J1118+48 (62 deg off the GP Lx < 1e36 erg/s at its peak) rises the suspicion that we may have so far missed a large population of BH in the galactic thick disc and/or halo. We wish to know whether there are fundamental differences between BH in the halo compared to BH in the disc. Furthermore some of these accreting BH in low mass X-ray binaries could be micro-blazars it is still an open question their possible relation to a subset of soft and variable unidentified EGRET sources that are spread at medium/high latitude most assembled within 30 deg from the Galactic Centre (GC). In the framework of Target of Opportunity (ToO) observations we aim to observe new BH XN at |b| > 5 deg not subject to INTEGRAL Core Program ToO altogether with multiwavelength observations with UV/opt/IR/radio telescopes. This proposal was submitted for AO 1 and AO 2 in correlation with XN in the galactic bulge approved by TAC with t [truncated! Please see actual data for full text]

银河系厚盘和/或晕中的黑洞（Black Hole, BH）会偶尔以具有极硬光谱的X射线新星（X-ray Nova, XN）形式出现。这些天体的起源是高能天体物理学中最引人入胜的问题之一：它们可能是从银道面（Galactic Plane, GP）被抛射出来的，或者是在星系盘形成之前于星系晕中形成的原始黑洞。在银纬|b|>5度的区域，黑洞X射线新星（BH XN）可能距离太阳较近、光学波段明亮且无遮挡，其致密射电对应体受到的星际散射较弱。本研究计划旨在：1）在全波段范围内探究吸积盘（accretion disc）不稳定性与相对论性喷流（relativistic jets）形成之间的关联；2）明确射电、红外及光学非热成分与伽马射线事件是否——正如近期在类星体中发现的那样——起源于相对论性喷流下游的同一激波区域；3）测定双星系统质心的空间速度，以了解这些黑洞的起源。XTE J1118+48（偏离银道面62度，峰值光度Lx<1e36 erg/s）的发现让人怀疑，我们至今可能遗漏了银河系厚盘和/或晕中的大量黑洞。我们希望了解晕中的黑洞与盘内的黑洞之间是否存在根本差异。此外，低质量X射线双星中的部分吸积黑洞可能是微耀变体（micro-blazars）——这仍是一个悬而未决的问题：它们是否与中/高纬度分布的一部分软且可变的未识别EGRET源存在关联，这些源大多集中在距离银心（Galactic Centre, GC）30度以内的区域。在机遇目标（Target of Opportunity, ToO）观测框架下，我们旨在观测|b|>5度且未被纳入INTEGRAL核心项目ToO的新黑洞X射线新星，并结合紫外/光学/红外/射电望远镜开展多波段观测。本提案曾针对AO1和AO2提交，与星系核球中的X射线新星相关，已获时间分配委员会（Time Allocation Committee, TAC）批准，但文本被截断！请查阅实际数据获取完整内容。